GRB 180728A and SN 2018fip: The nearest high-energy cosmological gamma-ray burst with an associated supernova

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Volume 708 (April 2026)

A&A, 708 (2026) A60

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Table 3.

Spectral energy distribution fit results.

Epochs	Model^c	χ²/d.o.f.	β_low	β_high	E_break	N_(H, int)^e	E(B − V)^e
(day)	–	–	–	–	(keV)	(10²¹ cm⁻²)	(mag)
0.03^a	BPL	1.10	$0 . 631_{- 0.005}^{+ 0.005}$ $Mathematical equation: $ 0.631_{-0.005}^{+0.005} $$	β_low + 0.5	$2 . 09_{- 0.05}^{+ 0.08}$ $Mathematical equation: $ 2.09_{-0.05}^{+0.08} $$	1.14	0.012
0.10^a	BPL	1.10	$0 . 592_{- 0.006}^{+ 0.008}$ $Mathematical equation: $ 0.592_{-0.006}^{+0.008} $$	β_low + 0.5	$2 . 63_{- 0.33}^{+ 0.42}$ $Mathematical equation: $ 2.63_{-0.33}^{+0.42} $$	1.14	0.012
0.03^b	PL	2.3	$0 . 59_{- 0.004}^{+ 0.006}$ $Mathematical equation: $ 0.59_{-0.004}^{+0.006} $$	–	–	1.14	0.012
0.10^b	PL	1.4	$0 . 62_{- 0.006}^{+ 0.006}$ $Mathematical equation: $ 0.62_{-0.006}^{+0.006} $$	–	–	1.14	0.012

0.24–1.50^d	PL	0.99	$0 . 705_{- 0.005}^{+ 0.004}$ $Mathematical equation: $ 0.705_{-0.005}^{+0.004} $$	–	–	$1 . 14_{- 0.28}^{+ 0.26}$ $Mathematical equation: $ 1.14_{-0.28}^{+0.26} $$	0.012 ± 0.009

Notes.

These two SEDs share extinction and dust absorption from later epochs, but the spectral-model parameters are left free.

Similar to ^a but using a single power law model.

We use two models: a broken power law (BPL) and a power law (PL).

Joint fit: These two SEDs share the same model, and only the normalisation is left free.

The first four SEDs have the same N_(H, int) and E(B − V), fixed to the values found in the late-time fit.

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